Abstract
Abstract In the first orbit of the Parker Solar Probe (PSP), in situ thermal plasma and magnetic field measurements were collected as close as 35 R Sun from the Sun, an environment that had not been previously explored. During the first orbit of PSP, the spacecraft flew through a streamer blowout coronal mass ejection (SBO-CME) on 2018 November 11 at 23:50 UT as it exited the science encounter. The SBO-CME on November 11 was directed away from the Earth and was not visible by L1 or Earth-based telescopes due to this geometric configuration. However, PSP and the STEREO -A spacecraft were able to make observations of this slow (v ≈ 380 km s−1) SBO-CME. Using the PSP data, STEREO-A images, and Wang–Sheeley–Arge model, the source region of the CME is found to be a helmet streamer formed between the northern polar coronal hole and a mid-latitude coronal hole. Using the YGUAZU-A model, the propagation of the CME is traced from the source at the Sun to PSP. This model predicts the travel time of the flux rope to the PSP spacecraft as 30 hr, which is within 0.33 hr of the actual measured arrival time. The in situ Solar Wind Electrons Alphas and Protons data were examined to determine that no shock was associated with this SBO-CME. Modeling of the SBO-CME shows that no shock was present at PSP; however, at other positions along the SBO-CME front, a shock could have formed. The geometry of the event requires in situ and remote sensing observations to characterize the SBO-CME and further understand its role in space weather.
Highlights
Coronal mass ejections (CMEs) originating at the Sun propagate in the heliosphere and drive space weather at the Earth
We have presented Parker Solar Probe (PSP) observations of an streamer blowout coronal mass ejection (SBO-CME) on 2018 November 11 starting at 23:50 UT
The SBOCME was seen in remote sensing observations by STA
Summary
Coronal mass ejections (CMEs) originating at the Sun propagate in the heliosphere and drive space weather at the Earth. The gravity and Lorentz forces are assumed to be negligible, meaning that the CME kinematics depend on the CME and solar wind conditions (speed and density) and the way they interchange momentum during their interaction (Vršnak 2001; Cantó et al 2005; Borgazzi et al 2009; Vršnak et al 2013, 2014) Any of these models can predict the travel time, speed, and density, but they cannot predict the in situ parameter time profiles that can be observed at any heliospheric distance. The focus of this paper is on utilizing the remote sensing and in situ data, as well as models, to understand the source, propagation, and lack of shock associated with the 2018 November 11 CME Other papers in this issue address the magnetic structure (Nieves-Chinchilla et al 2020) and energetic particles (Giacalone et al 2020) associated with this CME.
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